In Sec. , we study the GW emission from the scalar condensate. We first generalize the calculation framework in Ref. [1]} to include the subdominant modes. Then we check our formalism by calculating the GW emission luminosity for each of the four condensate modes in Sec. REF . The obtained results are consistent with previous calculations and analytic approximations. In Sec. REF , we calculate the GW emission with the interference of \(\lbrace 0,1,1\rbrace \)  and \(\lbrace 1,1,1\rbrace \)  modes. The interference term is suppressed by \(\sqrt{N_{111}/N_{011}}\) , where \(N_{nlm}\)  is the number of scalars in the \(\lbrace n,l,m\rbrace \)  mode. This mild suppression results in a sizeable beat-like pattern in the GW emission flux even when \(N_{111}/N_{011}\)  is small. This GW beat exists in the attractor phase of the \(\lbrace 1,1,1\rbrace \)  mode. We further study the strength and duration of the GW beat pattern for different initial parameters. In a pretty large parameter space, the GW beat is strong and lasts long enough to be observed (see Fig. REF ).
